TESS is capable of high precision measurements for this system due to the host star being bright (V=9.0 mag). However, TESS's large pixel size (21) is less than ideal for HD 80606 due to the presence of HD 80607, a nearby companion of similar spectral type and brightness (V=9.07 mag) separated by 20.5. Stellar blends dilute the transit signal causing a larger planet to mistakenly appear smaller [1]}, [2]}. In the reduction of TESS data, a wide aperture was used and includes light from both stars. Therefore, our estimate for the transit depth is underestimated. The estimated contamination is around \(\sim \) 48\(\%\)  and translates to a corrected transit depth \(\sim 2\times \)  greater than what we directly measure. Despite the contamination decreasing the transit depth, we still detect the transit at over 40 \(\sigma \)  which allows for a strong constraint on the time of mid-transit to within a few minutes (see Table REF  and Figure REF ).
